Black Hole evaporation in a thermalized final-state projection model

Details Black Hole evaporation in a thermalized final-state projection model Black Hole evaporation in a thermalized final-state projection model

2006-11-14

arxiv.org/abs/hep-th/0611152v1

Phys.Rev.D75:064009,2007

Physics

High Energy Physics

High Energy Physics - Theory

7 pages, 1 figure

Scientific paper

10.1103/PhysRevD.75.064009

We propose a modified version of the Horowitz-Maldacena final-state boundary condition based upon a matter-radiation thermalization hypothesis on the Black Hole interior, which translates into a particular entangled state with thermal Schmidt coefficients. We investigate the consequences of this proposal for matter entering the horizon, as described by a Canonical density matrix characterized by the matter temperature $T$. The emitted radiation is explicitly calculated and is shown to follow a thermal spectrum with an effective temperature $T_{eff}$. We analyse the evaporation process in the quasi-static approximation, highlighting important differences in the late stages with respect to the usual semiclassical evolution, and calculate the fidelity of the emitted Hawking radiation relative to the infalling matter.

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